Fig. REF  shows the resulting spectrum in the region of the H and K lines compared to an analogous synthetic spectrum from the BT-Settl model atmospheres [1]}, [2]}. Emission in the cores of the calcium lines is obvious and confirms that the system shows chromospheric activity. The spectrum was taken at orbital phase 0.9037 where the RV difference between the stars was 117 km s\(^{-1}\)  (approximately 3.5 pixels). The emission lines from the two stars overlap so it is not possible to assess the emission strengths from the two stars individually.
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